To probe the magnetic field morphology near the massive
young star Orion-IRc2, we used the BIMA array to map the
linear polarization of the J=2-1 SiO masers, in both the v=1
and v=0 vibrational levels, with 0.4'' angular resolution.

The strong v=1 masers are confined to a narrow zone 40 AU
from the star. These masers have fractional polarizations of
a few percent. The polarization position angle tends to
correlate with the maser intensity, and fluctuates on time
scales of years. For the v=1 masers the stimulated emission
rate R is much greater than the Zeeman splitting g\Omega
due to any plausible magnetic field, so the maser
polarization need not be correlated with the field
direction.

The much weaker v=0 masers originate 500 AU from IRc2, in
what appears to be a flared disk. For these masers we
measure a position angle PA~80\degr, constant in time
and varying little across the line profile. By contrast,
Tsuboi et al. (1996) measured PA~150\degr\ for the
J=1-0 v=0 SiO transition. Possibly this discrepancy is
attributable to Faraday rotation by plasma in the foreground
\ion{H}{2} region. If so, the intrinsic polarization angle
is ~55\degr, parallel to the plane of the circumstellar
disk. If the disk is seen edge-on, then the magnetic field
threads the disk poloidally, with relatively little pinch.